2001 Annual Science Report

NASA Jet Propulsion Laboratory Reporting  |  JUL 2000 – JUN 2001

Impact Frustration and Subsequent Generation of Biologically Tenable Climates on Earth and Mars

4 Institutions
3 Teams
0 Publications
0 Field Sites
Field Sites

Project Progress

Impact Frustration and Subsequent Generation of Biologically Tenable Climates on Earth and Mars (dm)

Mars is a water rich planet. Impact vaporization and melting studies of Mars subsurface H2O ice and computer simulation of crater ejecta demonstrate that most of the subsurface material sampled by visible impact craters appears to have contained some 5-30% by volume of water ice, indicating that the water mass on Mars is at least 3.9 ×10-4 times the mass of the planet. This compares to 2.8 × 10-4 in the case of the Earth.

Our analysis of the global acidification that occurred at the K/T boundary indicates that ~1 × 1017 equivalents of strong acid was deposited on the continents. We conclude that North America was preferably leached with greater densities of acid from prompt fallout of H2SO4 aerosol.

Shock temperatures measured in crystal calcite in the 95-160 GPa range yield radiative temperatures of 3300 to 5400 K. Calculations indicate that the temperatures are 400 to 1350 K lower than predictions indicating massive bond breakage under pressure. Calcite therefore decomposes upon unloading from only 18 GPa.

  • PROJECT INVESTIGATORS:
  • PROJECT MEMBERS:
    Thomas Ahrens
    Co-Investigator

    Satish Gupta
    Research Staff

    James Lyons
    Research Staff

    William Newman
    Research Staff

    John O'Keefe
    Research Staff

    Andy Shen
    Research Staff

    Sarah Stewart-Mukhopadhyay
    Undergraduate Student

  • RELATED OBJECTIVES:
    Objective 5.0
    Describe the sequences of causes and effects associated with the development of Earth's early biosphere and the global environment.

    Objective 8.0
    Search for evidence of ancient climates, extinct life and potential habitats for extant life on Mars.

    Objective 11.0
    Determine (theoretically and empirically) the ultimate outcome of the planet-forming process around other stars, especially the habitable ones.